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Observational Constraints on the Common Envelope Phase

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Abstract

The common envelope phase was first proposed more than 40 years ago to explain the origins of evolved, close binaries like cataclysmic variables. It is now believed that the phase plays a critical role in the formation of a wide variety of other phenomena ranging from type ia supernovae through to binary black holes, while common envelope mergers are likely responsible for a range of enigmatic transients and supernova imposters. Yet, despite its clear importance, the common envelope phase is still rather poorly understood. Here, we outline some of the basic principles involved, the remaining questions as well as some of the recent observational hints from common envelope phenomena—namely planetary nebulae and luminous red novae—which may lead to answering these open questions.

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Notes

  1. 1.

    This is roughly assuming that the orbital period distribution is not strongly dependent on the primary mass, which may not be the case [79].

  2. 2.

    The assumption that the current separation is equal to the immediately post-CE separation only holds for “young” systems, which have experienced negligible angular momentum loss since the CE. For older systems, one must account for the influence of disrupted magnetic braking on the observed orbital period [17].

  3. 3.

    This may only be the case if the CE occurs on the AGB. If the CE occurs while on the RGB, there are doubts as to whether the post-CE evolution of the exposed core would be fast enough to ionise the expanding envelope in time for it to be visible as a PN. However recent theoretical and observational efforts seem to indicate that these doubts are unfounded and that post-RGB PNe do indeed exist [36, 42].

  4. 4.

    The ejecta from luminous red novae, as discussed in Sect. 6, could also be used to study the CE ejection. However, these objects represent “failed” CEs, where the binary merged inside the CE (likely ejecting only a fraction of the envelope).

  5. 5.

    With lower fidelity data it can be difficult to distinguish between variability due to irradiation and variability due to ellipsoidal modulation, plausibly leading to a derived orbital period which is discrepant by a factor of two [3, 72].

  6. 6.

    The double-degenerate central star of NGC 1360 has an orbital period of ∼142 days [78], but may not be the result of a CE. Instead, such systems may evolve through stable, non-conservative mass transfer [121, 135] as described in Sect. 5.2.

  7. 7.

    The ages referred to here are kinematical ages and, as such, represent the minimum ages for each component (i.e. the age assuming that the material was ejected ballistically and has not been slowed by interaction with the surrounding interstellar medium).

  8. 8.

    Continuing with the unfortunate misnomers surrounding CE-related phenomena, just as planetary nebulae have no relation to planets, lumninous red novae are completely unrelated to classical novae or supernovae.

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Acknowledgements

DJ would like to thank the referee, Orsola De Marco, for her comprehensive report which improved both the clarity and completeness of this review.

DJ acknowledges support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU) and the European Regional Development Fund (FEDER) under grant AYA2017-83383-P. DJ also acknowledges support under grant P/308614 financed by funds transferred from the Spanish Ministry of Science, Innovation and Universities, charged to the General State Budgets and with funds transferred from the General Budgets of the Autonomous Community of the Canary Islands by the Ministry of Economy, Industry, Trade and Knowledge.

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  1. Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain

    David Jones

  2. Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Tenerife, Spain

    David Jones

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  1. Astronomical Institute of the Czech Academy of Sciences, Ondrejov, Czech Republic

    Petr Kabáth

  2. Instituto de Astrofisica de Canarias, La Laguna, Spain

    David Jones

  3. Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic

    Marek Skarka

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Jones, D. (2020). Observational Constraints on the Common Envelope Phase. In: Kabáth, P., Jones, D., Skarka, M. (eds) Reviews in Frontiers of Modern Astrophysics. Springer, Cham. https://doi.org/10.1007/978-3-030-38509-5_5

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